We combine 126 new galaxy-OVI absorber pairs from the CGM^2^ survey with 123 pairs drawn from the literature to examine the simultaneous dependence of the column density of OVI absorbers (N_OVI_) on galaxy stellar mass, star-formation rate, and impact parameter. The combined sample consists of 249 galaxy-OVI absorber pairs covering z=0-0.6, with host galaxy stellar masses M_*_=10^7.8^-10^11.2^M_{sun}_ and galaxy-absorber impact parameters R_{perp}_=0-400 proper kiloparsecs. In this work, we focus on the variation of N_OVI_ with galaxy mass and impact parameter among the star-forming galaxies in the sample. We find that the average N_OVI_ within one virial radius of a star-forming galaxy is greatest for star-forming galaxies with M_*_=10^9.2^-10^10^M_{sun}_. Star-forming galaxies with M* between 10^8^ and 10^11.2^M_{sun}_ can explain most OVI systems with column densities greater than 10^13.5^cm^-2^. Sixty percent of the OVI mass associated with a star-forming galaxy is found within one virial radius, and 35% is found between one and two virial radii. In general, we find that some departure from hydrostatic equilibrium in the CGM is necessary to reproduce the observed OVI amount, galaxy mass dependence, and extent. Our measurements serve as a test set for CGM models over a broad range of host galaxy masses.