Using the STAREVOL CODE, we provide an update of the Siess et al (2000) PMS grid with an up-to-date microphysic. The models' masses range from 0.2 to 1.5 Msun for four different metallicities. We also provide the rotating models for the same grid using different initial rotation rates. We carefully chosed a unique set of parameters for magnetised wind braking, disc-coupling and rotational mixing prescriptions that allows us to reproduce the rotation periods distributions measured in young open clusters and associations from PMS to the end of the MS. We'll show how these models behave comparatively to observations and the type of output that can be expected from the grid.