  Mass loss due to line-driven winds is central to our understanding of the
evolution of massive stars.
  We extend the evolution models introduced in Paper I, where the mass loss
recipe is based on the simultaneous calculation of the wind hydrodynamics and
the line-acceleration, by incorporating the effects of stellar rotation. We
introduce a grid of self-consistent line-force parameters for a set of standard
evolutionary tracks. With that, we generate a new set of evolutionary tracks
with rotation for $M_\text{ZAMS}=25,40,70,$ and $120\,M_\odot$, and
metallicities $Z=0.014$ and $0.006$.
  The self-consistent approach gives lower mass loss rates than the standard
values adopted in previous evolution models. This decrease impacts strongly on
the tracks of the most massive models. Weaker winds allow the star to retain
more mass, but also more angular momentum. As a consequence, weaker wind models
rotate faster and show a less efficient mixing in their inner stellar
structure.
  The new tracks predict an evolution of the rotational velocities through the
MS in close agreement with the range of $\varv\sin i$ values found by recent
surveys of Galactic O-type stars. As subsequent implications, the weaker winds
from self-consistent models suggest a reduction of the contribution of the
isotope $^{26}$Al to the ISM due to stellar winds of massive stars during the
MS phase. Moreover, the higher luminosities found for the self-consistent
evolutionary models suggest that some populations of massive stars might be
less massive than previously thought, as in the case of Ofpe stars at the
Galactic Centre. Therefore, this study opens a wide range of consequences for
further research based on the evolution of massive stars.
