Comparison of the molecular gas properties, part II. Left panels: molecular gas mass (M_H2) versus the offset from the MS (derived assuming the relation by Sargent et al. 2014; top panel) and host-galaxy dust mass (M_dust; bottom panel). Seyfert 2 galaxies are shown with red diamonds, and the control sample is represented by gray circles (DustPedia) and green squares (Co19). Bottom panel: we show the M_H2 − M_dust diagram, where the M_H2 of the 33 5MUSES SFGs were derived from the CO luminosity (Co19), assuming α_CO = 4.3 M_⊙ pc⁻² (K km s⁻¹)⁻¹. We do not represent the entire sample of 5MUSES SFGs since their are derived from the M_dust assuming a dust-to-gas ratio (GDR). For purely illustrative purposes, the best-fit trend (dashed black line) for the control sample of inactive galaxies is shown, and the two dotted black lines are the same trend shifted by a factor of 0.5 dex in either direction. The best-fit slope (α) and normalization (β) are reported in each panel. Right column: same scaling relations presented on the left, but with binned values (using the same method as in Fig. 5). The red-shaded regions are as described in Fig. 5.