Studies of the galaxy clustering at low and intermediate redshifts show that the relation between the luminous structure and underlying dark matter distribution is not only biased but also dependent on properties of galaxies. To understand the origin of this separation the studies need to be conducted on spectroscopic data at higher redshift. With this aim in mind, we studied the dependence of galaxy clustering on their luminosity and stellar mass in the redshift range between 2 and 3.5 using spectroscopic data from the VIMOS Ultra Deep Survey (VUDS). We measured how the dependence of characteristic dark matter halo masses, large scale bias and halo asymmetry changes with both redshift and galaxy properties. We measured the stellar-to-halo mass ratio (SHMR) which points to a significant model-observation discrepancy for low-mass galaxies at z~3, suggesting a higher than expected star formation efficiency of these galaxies.