  We present the study of the dependence of galaxy clustering on luminosity and
stellar mass in the redshift range 2$<$z$<$3.5 using 3236 galaxies with robust
spectroscopic redshifts from the VIMOS Ultra Deep Survey (VUDS). We measure the
two-point real-space correlation function $w_p(r_p)$ for four volume-limited
stellar mass and four luminosity, M$_{UV}$ absolute magnitude selected,
sub-samples. We find that the scale dependent clustering amplitude $r_0$
significantly increases with increasing luminosity and stellar mass indicating
a strong galaxy clustering dependence on these properties. This corresponds to
a strong relative bias between these two sub-samples of $\Delta$b/b$^*$=0.43.
Fitting a 5-parameter HOD model we find that the most luminous and massive
galaxies occupy the most massive dark matter haloes with
$\langle$M$_h$$\rangle$ = 10$^{12.30}$ h$^{-1}$ M$_{\odot}$. Similar to the
trends observed at lower redshift, the minimum halo mass M$_{min}$ depends on
the luminosity and stellar mass of galaxies and grows from M$_{min}$
=10$^{9.73}$ h$^{-1}$M$_{\odot}$ to M$_{min}$=10$^{11.58}$ h$^{-1}$M$_{\odot}$
from the faintest to the brightest among our galaxy sample, respectively. We
find the difference between these halo masses to be much more pronounced than
is observed for local galaxies of similar properties. Moreover, at z~3, we
observe that the masses at which a halo hosts, on average, one satellite and
one central galaxy is M$_1$$\approx$4M$_{min}$ over all luminosity ranges,
significantly lower than observed at z~0 indicating that the halo satellite
occupation increases with redshift. The luminosity and stellar mass dependence
is also reflected in the measurements of the large scale galaxy bias, which we
model as b$_{g,HOD}$($>$L)=1.92+25.36(L/L$^*$)$^{7.01}$. We conclude our study
with measurements of the stellar-to-halo mass ratio (SHMR).
