We present updated results constraining multiplicity demographics for the stellar and substellar population of the Orion Nebula Cluster (ONC), across primary masses 0.012 - 0.7 Msun. Our study utilizes archival Hubble Space Telescope (HST) data obtained with the Advanced Camera for Surveys (ACS) using multiple filters (PID: 10246, PI M. Robberto). Studying the companion populations of young, star-forming regions provides valuable constraints of how the birth environment affects multiple formation and evolution. Previous multiplicity surveys in Taurus (a low-mass, low-density association) identify a companion frequency to low-mass primary stars roughly twice that of the Galactic field, over all mass ratios and for separations of 3-5000 au. Our study investigates the companion population of the ONC (a high-mass, high density star-forming region) where dynamical interactions are more likely to occur and modify the companion population. Our study is sensitive to companions beyond orbital separations of 10 au (0.025”, 0.5λ/D at 555nm) using a double point-spread function (PSF) fitting algorithm with empirical, position-dependent PSF models. We have identified 44 companions to low-mass stars and 7 companions to sub-stellar primaries. We found: 1) the companion frequency (CF) of low-mass stars in the ONC is consistent with the Galactic field over all mass ratios and orbital separations of 10-200 au, in contrast to the higher CF found in low-density regions like Taurus, 2) the power-law fit to the mass ratio distribution of low-mass stellar primaries in the ONC is consistent with that of the field and Taurus, similar to results from N-body simulations and potentially indicative of a universal formation mechanism, and 3) the CF to brown dwarfs for separations > 20 au in the ONC is in excess of the field, requiring further dynamical evolution to destroy binaries with low binding energy to resemble the field.