  Supernova (SN) 2017cbv in NGC 5643 is one of a handful of type Ia supernovae
(SNe~Ia) reported to have excess blue emission at early times. This paper
presents extensive $BVRIYJHK_s$-band light curves of SN 2017cbv, covering the
phase from $-16$ to $+125$ days relative to $B$-band maximum light. SN 2017cbv
reached a $B$-band maximum of 11.710$\pm$0.006~mag, with a post-maximum
magnitude decline $\Delta m_{15}(B)$=0.990$\pm$0.013 mag. The supernova
suffered no host reddening based on Phillips intrinsic color, Lira-Phillips
relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus
$\mu=30.58\pm0.05$~mag and assuming $H_0$=72~$\rm km \ s^{-1} \ Mpc^{-1}$, we
found that 0.73~\msun $^{56}$Ni was synthesized during the explosion of SN
2017cbv, which is consistent with estimates using reddening-free and
distance-free methods via the phases of the secondary maximum of the NIR-band
light curves. We also present 14 near-infrared spectra from $-18$ to $+49$~days
relative to the $B$-band maximum light, providing constraints on the amount of
swept-up hydrogen from the companion star in the context of the single
degenerate progenitor scenario. No $Pa{\beta}$ emission feature was detected
from our post-maximum NIR spectra, placing a hydrogen mass upper limit of 0.1
$M_{\odot}$. The overall optical/NIR photometric and NIR spectral evolution of
SN 2017cbv is similar to that of a normal SN~Ia, even though its early
evolution is marked by a flux excess no seen in most other well-observed normal
SNe~Ia. We also compare the exquisite light curves of SN 2017cbv with some
$M_{ch}$ DDT models and sub-$M_{ch}$ double detonation models.
