  We present optical and near-infrared light curves and optical spectra of SN
2013dx, associated with the nearby (redshift 0.145) gamma-ray burst GRB
130702A. The prompt isotropic gamma-ray energy released from GRB 130702A is
measured to be $E_{\gamma,iso}=6.4_{-1.0}^{+1.3}\times10^{50}$erg (1keV-10MeV
in the rest frame), placing it intermediate between low-luminosity GRBs like
GRB 980425/SN 1998bw and the broader cosmological population. We compare the
observed $g'r'i'z'$ light curves of SN 2013dx to a SN 1998bw template, finding
that SN 2013dx evolves ~20% faster (steeper rise time), with a comparable peak
luminosity. Spectroscopically, SN 2013dx resembles other broad-lined Type Ic
supernovae, both associated with (SN 2006aj and SN 1998bw) and lacking (SN
1997ef, SN 2007I, and SN 2010ah) gamma-ray emission, with photospheric
velocities around peak of ~21,000km s$^{-1}$. We construct a quasi-bolometric
($g'r'i'z'yJ$) light curve for SN 2013dx, only the fifth GRB-associated SN with
extensive NIR coverage and the third with a bolometric light curve extending
beyond $\Delta t>40$d. Together with the measured photospheric velocity, we
derive basic explosion parameters using simple analytic models. We infer a
$^{56}$Ni mass of $M_{\mathrm{Ni}}=0.37\pm0.01$M$_{\odot}$, an ejecta mass of
$M_{\mathrm{ej}}=3.1\pm0.1$M$_{\odot}$, and a kinetic energy of
$E_{\mathrm{K}}=(8.2\pm0.43)\times10^{51}$ erg (statistical uncertainties
only), consistent with previous GRB-associated SNe. When considering the
ensemble population of GRB-associated SNe, we find no correlation between the
mass of synthesized $^{56}$Ni and high-energy properties, despite clear
predictions from numerical simulations that $M_{\mathrm{Ni}}$ should correlate
with the degree of asymmetry. On the other hand, $M_{\mathrm{Ni}}$ clearly
correlates with the kinetic energy of the supernova ejecta across a wide range
of core-collapse events.
