  We present an analysis of Type Ia Supernovae (SNe~Ia) from both the Carnegie
Supernova Project~I (CSP-I) and II (CSP-II), and extend the Hubble diagram from
the optical to the near-infrared wavelengths ($uBgVriYJH$). We calculate the
Hubble constant, $H_0$, using various distance calibrators: Cepheids, Tip of
the 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 $\rm
H_0=73.22 \pm 0.68 \ (stat) \pm 1.28 \ (sys) \ km \ s^{-1} \ Mpc^{-1}$ 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 of
the 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-only
uncertainty, the tension between the late-time $H_0$ we derive by combining the
various distance calibrators and the early-time $H_0$ from the Cosmic Microwave
Background is reduced. The highest precision in SN~Ia luminosity is found in
the $Y$ band ($0.12\pm0.01$ mag), as defined by the intrinsic scatter
($\sigma_{int}$). We revisit SN~Ia Hubble residual-host mass correlations and
recover previous results that these correlations do not change significantly
between the optical and the near-infrared wavelengths. Finally, SNe~Ia that
explode beyond 10 kpc from their host centers exhibit smaller dispersion in
their luminosity, confirming our earlier findings. Reduced effect of dust in
the outskirt of hosts may be responsible for this effect.
