Aims. We study the impact of internal gravity waves (IGW), meridio nal circulation, shear turbulence, and stellar contractio n on the internal rotation profile and surface velocity evolution of s lar metallicity low-mass pre-main sequence stars. Methods. We compute a grid of rotating stellar evolution models with m asses between 0.6 and 2.0 M ⊙ taking these processes into account for the transport of angular momentum, as soon as the radiative core appears and assuming no more disk-locking fr om that moment on. IGW generation along the PMS is computed taking Re ynolds-stress and buoyancy into account in the bulk of the st ellar convective envelope and convective core (when present). Re distribution of angular momentum within the radiative laye rs accounts for damping of prograde and retrograde IGW by thermal di ffus vity and viscosity in corotation resonance. Results. Over the whole mass range considered, IGW are found to be e fficiently generated by the convective envelope and to slow down the stellar core early on the PMS. In stars more massive t han∼ 1.6 M⊙, IGW produced by the convective core also contribute to angular momentum redistribution close to the ZAMS. Conclusions. Overall, IGW are found to significantly change the internal r otation profile of PMS low-mass stars.