The SFR−density relation in the VUDS+ sample as a function of stellar mass. Left: as in the left panel of Fig. 5, the SFR–δ_gal relation for our final VUDS+ sample, but now with galaxies broken up into three approximately equally-sized samples binned in stellar mass using the limits indicated at the bottom right of the panel. The points and their associated uncertainties have the same meaning as in Fig. 5. The solid vertical lines and their meanings are the same as in Fig. 5. A weak but significant positive correlation between SFR and log(1 + δ_gal) is seen in the two lower mass bins. A stronger and equally significant positive correlation is seen for the highest stellar mass galaxies and is especially apparent in the Peak Region. Right: distribution of the logarithmic value of the likelihood of no correlation between SFR and log(1 + δ_gal) of our final spectral sample for the three different stellar mass bins used in our analysis for the full redshift range 2 ≤ z ≤ 5. This distribution is calculated from 1000 Monte Carlo realization in which we perturb each SFR and log(1 + δ_gal) value by their associated errors. These histograms do not meaningfully change if we additionally include dusty star-forming galaxies with high rates of SFR and galaxies with no active star formation, both of which are completely missed in our sample, at proportions appropriate for their number density at 2 ≤ z ≤ 5 in our Monte Carlo simulations. For reference, a log(likelihood) < −2.5 corresponds to a positive correlation between the two parameters estimated at ≥3σ confidence level.