  We examine the properties of Wolf--Rayet (WR) stars predicted by models of
rotating stars taking account of the new mass loss rates for O--type stars and
WR stars (Vink et al. \cite{Vink00}, \cite{Vink01}; Nugis & Lamers
\cite{NuLa00}) and of the wind anisotropies induced by rotation. We find that
the rotation velocities $v$ of WR stars are modest, i.e. about 50 km s$^{-1}$,
not very dependant on the initial $v$ and masses. For the most massive stars,
the evolution of $v$ is very strongly influenced by the values of the mass loss
rates; below $\sim$12 M$_\odot$ the evolution of rotation during the MS phase
and later phases is dominated by the internal coupling. Massive stars with
extreme rotation may skip the LBV phase.
  Models having a typical $v$ for the O--type stars have WR lifetimes on the
average two times longer than for non--rotating models. The increase of the WR
lifetimes is mainly due to that of the H--rich eWNL phase. Rotation allows a
transition WN/WC phase to be present for initial masses lower than 60
M$_\odot$. The durations of the other WR subphases are less affected by
rotation. The mass threshold for forming WR stars is lowered from 37 to 22
M$_\odot$ for typical rotation. The comparisons of the predicted number ratios
WR/O, WN/WC and of the number of transition WN/WC stars show very good
agreement with models with rotation, while this is not the case for models with
the present--day mass loss rates and no rotation. As to the chemical abundances
in WR stars, rotation brings only very small changes for WN stars, since they
have equilibrium CNO values. However, WC stars with rotation have on average
lower C/He and O/He ratios. The luminosity distribution of WC stars is also
influenced by rotation.
