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Although the role of magnetic fields in launching molecular outflows inmassive YSOs has been convincingly demonstrated by theoretical arguments,observationally, the alignment of the magnetic field lines with the molecularoutflows is still under debate. We aim to complete the measurements of thedirection of the magnetic fields at mas resolution around a sample of massivestar-forming regions (MSFRs) to determine whether the magnetic field andoutflows are aligned. In 2012, we started a large VLBI campaign with the EVN tomeasure the magnetic field orientation and strength toward a sample of 31 MSFRs(the flux-limited sample) by analyzing the polarized emission of 6.7GHz CH3OHmasers. In the previous papers of the series, we have presented 80% of thesample. Here, we report the linearly and circularly polarized emission of6.7GHz CH3OH masers toward the last five MSFRs of the flux-limited sample. Thesources are G30.70-0.07, G30.76-0.05, G31.28+0.06, G32.03+0.06, andG69.52-0.97. We detected a total of 209 masers, 15% of which show linearlypolarized emission (0.07%-16.7%), and 2% of which show circularly polarizedemission (0.2%-4.2%). Zeeman splitting was measured toward G30.70-0.07,G32.03+0.06, and G69.52-0.97. The statistical analysis of the entireflux-limited sample shows that the observations are consistent with a bimodaldistribution in the difference between the 3D magnetic field direction and theoutflow axis, with half the magnetic field directions being perpendicular andthe other half being parallel to the outflow. In addition, we determined thattypical values of the linear and circular polarization fractions for 6.7 GHzCH3OH masers are Pl=1.0%-2.5% and Pv=0.5%-0.75%, respectively. We found that atypical Zeeman splitting is in the range between 0.5 m/s and 2.0 m/s. Thiswould correspond to 9 mG<$|B_{||}|$<40 mG if F=3->4 is the most favoredhyperfine transition.

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions. V. Completion of the flux-limited sample