Even though SN 2012cg is one of the best-studied Type Ia Supernovae to date, the nature of its progenitor system has been debated in numerous studies. Specifically, it is difficult to reconcile recent claims of the detection of a $sim 6 rm{M}_odot$ main-sequence companion with recent deep, late-time H$alpha{}$ flux limits. In this study we add three new constraints: 1) We analyze new high-signal-to-noise, nebular-phase, LBT/MODS spectrum of SN 2012cg and place an upper limit on the amount of low-velocity, solar-abundance material removed from a possible companion of $ < 7.8 times 10^{-3} rm{M}_odot$. 2) We use Swift X-ray observations to constrain the preexplosion mass-loss rate to be $dot M<10^{-6},$ $rm{M}_odot$ yr$^{-1}$ for $v_textrm{w}=100,rm{km,s^{-1}}$. 3) We carefully reanalyze a prediscovery MASTER image and, with published light curves of SN 2012cg, we estimate the time of first light and conservatively constrain the radius of a Roche-lobe overflowing companion to be $< 0.24 rm{R}_odot$. These observations disagree with a large nearby companion, and, when considered with other studies of SN 2012cgs progenitor system, essentially rule out a non-degenerate companion.
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