We measure the molecular-to-atomic gas ratio,
Rmol, and the star formation rate (SFR) per unit molecular gas mass, SFEmol, in 38 nearby galaxies selected from the Virgo Environment Traced in CO (VERTICO) survey. We stack ALMA 12CO ( J= 2−1) spectra coherently using H ivelocities from the VIVA survey to detect faint CO emission out to galactocentric radii rgal ∼ 1.2 r25. We determine the scale lengths for the molecular and stellar components, finding a ∼3:5 relation compared to ∼1:1 in field galaxies, indicating that the CO emission is more centrally concentrated than the stars. We compute Rmol as a function of different physical quantities. While the spatially resolved Rmol on average decreases with increasing radius, we find that the mean molecular-to-atomic gas ratio within the stellar effective radius R e, Rmol( r< R e), shows a systematic increase with the level of H i, truncation and/or asymmetry (HI perturbation). Analysis of the molecular- and the atomic-to-stellar mass ratios within R e, R e, SFEmol( r< Re), with increasingly perturbed H i. Therefore, compared to field galaxies from the field, VERTICO galaxies are more compact in CO emission in relation to their stellar distribution, but increasingly perturbed atomic gas increases their Rmol and decreases the efficiency with which their molecular gas forms stars.