  We present and perform a detailed analysis of multi-wavelength observations
of \thisgrb, an optical bright GRB with an observed reverse shock (RS)
signature. Observations of this GRB were acquired with the BOOTES-4 robotic
telescope, the \fermi, and the \swift missions. Time-resolved spectroscopy of
the prompt emission shows that changes to the peak energy (\Ep) tracks
intensity and the low-energy spectral index seems to follow the intensity for
the first episode, whereas this tracking behavior is less clear during the
second episode. The fit to the afterglow light curves shows that the early
optical afterglow can be described with RS emission and is consistent with the
thin shell scenario of the constant ambient medium. The late time afterglow
decay is also consistent with the prediction of the external forward shock (FS)
model. We determine the properties of the shocks, Lorentz factor, magnetization
parameters, and ambient density of \thisgrb, and compare these parameters with
another 12 GRBs, consistent with having RS produced by thin shells in an
ISM-like medium. The value of the magnetization parameter ($R_{\rm B} \approx
18$) indicates a moderately magnetized baryonic dominant jet composition for
\thisgrb. We also report the host galaxy photometric observations of \thisgrb
obtained with 10.4m GTC, 3.5m CAHA, and 3.6m DOT telescopes and find the host
(photo $z$ = $2.8^{+0.7}_{-0.9}$) to be a high mass, star-forming galaxy with a
star formation rate of $20 \pm 10 \msun$ $\rm yr^{-1}$.
