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Star formation activity in the central molecular zone (CMZ) directly manifests itself as radio continuum free-free emission (Bremsstrahlung) and radio recombination line emission from H II regions surrounding newly formed massive stars. We derive the overall distribution of the H II regions and their fundamental properties: electron temperature (<inline-formula><tex-math id="TM0001" notation="LaTeX">$T_{\rm e}$</tex-math></inline-formula>) and emission measure (EM), and hence electron density in the form of two-dimensional distribution maps over the CMZ by analyzing the ACES (ALMA CMZ Exploration Survey) H40<inline-formula><tex-math id="TM0002" notation="LaTeX">$\alpha$</tex-math></inline-formula> (99.02 GHz) recombination line and 99.6 GHz continuum emission data with synthesized beam widths of <inline-formula><tex-math id="TM0003" notation="LaTeX">$2{_{.}^{\prime\prime}} 45$</tex-math></inline-formula> (0.097 pc at 8.2 kpc) and <inline-formula><tex-math id="TM0004" notation="LaTeX">$2{_{.}^{\prime\prime}} 14$</tex-math></inline-formula>, respectively. We apply the "TeEM" method (<inline-formula><tex-math id="TM0005" notation="LaTeX">$T_{\rm e}$</tex-math></inline-formula>-EM mapping), which creates <inline-formula><tex-math id="TM0006" notation="LaTeX">$T_{\rm e}$</tex-math></inline-formula> and EM maps from input 2D maps of the continuum and integrated line intensity. The analysis covers the entire ACES field from <inline-formula><tex-math id="TM0007" notation="LaTeX">$l\sim -{0{_{.}^{\circ}}6}$</tex-math></inline-formula> to <inline-formula><tex-math id="TM0008" notation="LaTeX">${+0.^{\!\!\circ}8}$</tex-math></inline-formula> and from <inline-formula><tex-math id="TM0009" notation="LaTeX">$b\sim -0.^{\!\!\circ} 2$</tex-math></inline-formula> to <inline-formula><tex-math id="TM0010" notation="LaTeX">$+0.^{\!\!\circ} 1$</tex-math></inline-formula>. The area analyzed is complete and includes previously known H II regions such as Sgr B2, Sgr B1, the Sickle, the Pistol, thermal filaments (Bridges), Sgr A H II regions, the Minispiral, and many other known H II regions. Sgr C is not included in the analysis due to the insufficient signal-to-noise ratio in the recombination line map. The mean electron temperature over the CMZ is determined to be <inline-formula><tex-math id="TM0011" notation="LaTeX">$\langle T_{\rm e} \rangle _{\rm CMZ}= 5872 \pm 78 ~{\rm (SE)} ~\pm 3682~{\rm (SD)}$</tex-math></inline-formula> K (SE: standard error of the mean, SD: pixel-to-pixel standard deviation). Some H II regions, such as Sgr B2 Main and the Minispiral, exhibit large scatter and an internal <inline-formula><tex-math id="TM0012" notation="LaTeX">$T_{\rm e}$</tex-math></inline-formula> gradient of several thousand K per parsec. The EM distribution is more diverse, varying by orders of magnitude from <inline-formula><tex-math id="TM0013" notation="LaTeX">${\sim }10^5$</tex-math></inline-formula> to <inline-formula><tex-math id="TM0014" notation="LaTeX">${\sim }3\times 10^8$</tex-math></inline-formula> pc cm<inline-formula><tex-math id="TM0015" notation="LaTeX">$^{-6}$</tex-math></inline-formula> within the CMZ, as well as within individual H II regions.