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We present an analysis of Type Ia Supernovae (SNe~Ia) from both the CarnegieSupernova Project~I (CSP-I) and II (CSP-II), and extend the Hubble diagram fromthe optical to the near-infrared wavelengths ($uBgVriYJH$). We calculate theHubble constant, $H_0$, using various distance calibrators: Cepheids, Tip ofthe Red Giant Branch (TRGB), and Surface Brightness Fluctuations (SBF).Combining all methods of calibrations, we derive $\rm H_0=71.76 \pm 0.58 \(stat) \pm 1.19 \ (sys) \ km \ s^{-1} \ Mpc^{-1}$ from $B$-band, and $\rmH_0=73.22 \pm 0.68 \ (stat) \pm 1.28 \ (sys) \ km \ s^{-1} \ Mpc^{-1}$ from$H$-band. By assigning equal weight to the Cepheid, TRGB, and SBF calibrators,we derive the systematic errors required for consistency in the first rung ofthe distance ladder, resulting in a systematic error of $1.2\sim 1.3 \rm \ km \s^{-1} \ Mpc^{-1}$ in $H_0$. As a result, relative to the statistics-onlyuncertainty, the tension between the late-time $H_0$ we derive by combining thevarious distance calibrators and the early-time $H_0$ from the Cosmic MicrowaveBackground is reduced. The highest precision in SN~Ia luminosity is found inthe $Y$ band ($0.12\pm0.01$ mag), as defined by the intrinsic scatter($\sigma_{int}$). We revisit SN~Ia Hubble residual-host mass correlations andrecover previous results that these correlations do not change significantlybetween the optical and the near-infrared wavelengths. Finally, SNe~Ia thatexplode beyond 10 kpc from their host centers exhibit smaller dispersion intheir luminosity, confirming our earlier findings. Reduced effect of dust inthe outskirt of hosts may be responsible for this effect.

Carnegie Supernova Project-I and -II: Measurements of $H_0$ using Cepheid, TRGB, and SBF Distance Calibration to Type Ia Supernovae