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, \mathrm { iso } } = 6.4 _ { -1.0 } ^ { +1.3 } \times 10 ^ { 50 } erg ( 1 keV to 10 MeV 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 ^ { \prime } r ^ { \prime } i ^ { \prime } z ^ { \prime } light curves of SN 2013dx to a SN 1998bw template , finding that SN 2013dx evolves \sim 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 \sim 21,000 km s ^ { -1 } . We construct a quasi-bolometric ( g ^ { \prime } r ^ { \prime } i ^ { \prime } z ^ { \prime } yJ ) light curve for SN 2013dx , only the fifth GRB-associated SN with extensive near-infrared 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 \pm 0.01 M _ { \odot } , an ejecta mass of M _ { \mathrm { ej } } = 3.1 \pm 0.1 M _ { \odot } , and a kinetic energy of E _ { \mathrm { K } } = ( 8.2 \pm 0.43 ) \times 10 ^ { 51 } erg ( statistical uncertainties only ) , consistent with previous GRB-associated supernovae . When considering the ensemble population of GRB-associated supernovae , 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 .