  We study the impact of internal gravity waves (IGW), meridional circulation,
shear turbulence, and stellar contraction on the internal rotation profile and
surface velocity evolution of solar metallicity low-mass pre-main sequence
stars. We compute a grid of rotating stellar evolution models with masses
between 0.6 and 2.0Msun taking these processes into account for the transport
of angular momentum, as soon as the radiative core appears and assuming no more
disk-locking from that moment on.IGW generation along the PMS is computed
taking Reynolds-stress and buoyancy into account in the bulk of the stellar
convective envelope and convective core (when present). Redistribution of
angular momentum within the radiative layers accounts for damping of prograde
and retrograde IGW by thermal diffusivity and viscosity in corotation
resonance. Over the whole mass range considered, IGW are found to be
efficiently generated by the convective envelope and to slow down the stellar
core early on the PMS. In stars more massive than ~ 1.6Msun, IGW produced by
the convective core also contribute to angular momentum redistribution close to
the ZAMS. Overall, IGW are found to significantly change the internal rotation
profile of PMS low-mass stars.
