Results. We report very strong differences in the disk fractions of low-mass stars and brown dwarfs (similar to 58%) when compared to higher mass stars (26(3)(+4)% ), with 0.6 M-circle dot being the critical mass we find for this dichotomy. As a byproduct, we address the implications of the spatial distribution of disk and diskless members in the formation scenario of the cluster itself. We used the Ha emission to distinguish among accreting and non-accreting sources, finding that 38(-7)(+8)% of sources harboring disks undergo active accretion and that his percentage stays similar in the substellar regime. For these sources we have estimated accretion rates. Finally, regarding rotational velocities, we find a high dispersion in nu sin(i) that is even higher among the diskless population.