We present new NuSTAR and Chandra observations of NGC 3393 , a galaxy reported to host the smallest separation dual AGN resolved in the X-rays . While past results suggested a 150 pc separation dual AGN , three times deeper Chandra imaging , combined with adaptive optics and radio imaging suggest a single , heavily obscured , radio-bright AGN . Using VLA and VLBA data , we find an AGN with a two-sided jet rather than a dual AGN and that the hard X-ray , UV , optical , NIR , and radio emission are all from a single point source with a radius < 0.2 ^ { \prime \prime } . We find that the previously reported dual AGN is most likely a spurious detection resulting from the low number of X-ray counts ( < 160 ) at 6-7 keV and Gaussian smoothing of the data on scales much smaller than the PSF ( 0.25 ^ { \prime \prime } vs. 0.80 ^ { \prime \prime } FWHM ) . We show that statistical noise in a single Chandra PSF generates spurious dual peaks of the same separation ( 0.55 \pm 0.07 { \mbox { $ { } ^ { \prime \prime } $ } } vs. 0.6 ^ { \prime \prime } ) and flux ratio ( 39 \pm 9 \% vs. 32 % counts ) as the purported dual AGN . With NuSTAR , we measure a Compton-thick source ( N _ { H } = 2.2 \pm 0.4 \times 10 ^ { 24 }  { \thinspace cm } ^ { -2 } ) with a large torus half-opening angle , \theta _ { tor } = 79 _ { -19 } ^ { +1 } { \mbox { $ { } ^ { \circ } $ } } which we postulate results from feedback from strong radio jets . This AGN shows a 2-10 keV intrinsic to observed flux ratio of \approx 150 ( L _ { 2 - 10 \ > \mathrm { keV\ > int } } = 2.6 \pm 0.3 \times 10 ^ { 43 } \hbox { $ { \thinspace erg } % { \thinspace s } ^ { -1 } $ } vs. L _ { 2 - 10 \ > \mathrm { keV\ > observed } } = 1.7 \pm 0.2 \times 10 ^ { 41 } \hbox { $ { \thinspace erg% } { \thinspace s } ^ { -1 } $ } ) . Using simulations , we find that even the deepest Chandra observations would severely underestimate the intrinsic luminosity of NGC 3393 above z > 0.2 , but would detect an unobscured AGN of this luminosity out to high redshift ( z \approx 5 ) .