  We present ground-based and HST optical and infrared observations of XRF
100316D / SN 2010bh. It is seen that the optical light curves of SN 2010bh
evolve at a faster rate than the archetype GRB-SN 1998bw, but at a similar rate
to SN 2006aj, a supernova that was spectroscopically linked with XRF 060218,
and at a similar rate to non-GRB associated type Ic SN 1994I. We estimate the
rest-frame extinction of this event from our optical data to be E(B-V)=0.18 +/-
0.08 mag. We find the V-band absolute magnitude of SN 2010bh to be M_{V}=-18.62
+/- 0.08, which is the faintest peak V-band magnitude observed to-date for a
spectroscopically-confirmed GRB-SNe. When we investigate the origin of the flux
at t-t_{o}=0.598 days, it is shown that the light is not synchrotron in origin,
but is likely coming from the supernova shock break-out. We then use our
optical and infrared data to create a quasi-bolometric light curve of SN 2010bh
which we model with a simple analytical formula. The results of our modeling
imply that SN 2010bh synthesized a nickel mass of M_{Ni} \approx 0.10 M_{sun},
ejected M_{ej} \approx 2.2 M_{sun} and has an explosion energy of E_{k} \approx
1.4 x 10^{52} erg. Finally, for a sample 22 GRB-SNe we check for a correlation
between the stretch factors and luminosity factors in the R band and conclude
that no statistically-significant correlation exists.
