Recent analysis of the rotation of stars in young clusters show some patterns related to the age and mass of their members. These patterns seem to be related to internal changes due to the stellar evolution (moment of inertia, development of a radiative core) and external influences (presence of a disk, topology of the stellar magnetic field, etc). In this work we try to capture this evolution through Monte Carlo simulations of synthetic stellar clusters. We simulate two groups of stars, with different mass intervals, from brown dwarfs and very low mass stars in the first group, to solar mass stars in the second group. We explore the relation between rotation and the presence of an accretion disk. We also play with angular momentum conditions, from conservation to loss by a stellar magnetic wind. Our results show that, for solar type stars, the conservation of the rotation period while the accretion disk is present (disk locking) and the conservation of angular momentum after this are able to reproduce the observations of clusters younger than 20 Myrs. We reproduce the bimodal behavior in which diskless stars rotate faster than disk stars. For older clusters, it is necessary to introduce the loss of angular momentum by a stellar magnetic wind. However, in this case, the agreement with the observations is not so good. We have to consider the angular momentum exchange between the radiative core and the convective envelope. For brown dwarfs and very low mass stars, we see that disk locking is not so important and the rotational behavior is different from what is seen in their solar mass counterparts.