The evolution of clustering length, large-scale bias and host halo mass
  at 2<z<5 in the VIMOS Ultra Deep Survey (VUDS)
  We investigate the evolution of galaxy clustering for galaxies in the
redshift range 2.0<$z$<5.0 using the VIMOS Ultra Deep Survey (VUDS). We present
the projected (real-space) two-point correlation function $w_p(r_p)$ measured
by using 3022 galaxies with robust spectroscopic redshifts in two independent
fields (COSMOS and VVDS-02h) covering in total 0.8 deg$^2$. We quantify how the
scale dependent clustering amplitude $r_0$ changes with redshift making use of
mock samples to evaluate and correct the survey selection function. Using a
power-law model $\xi(r) = (r/r_0)^{-\gamma}$ we find that the correlation
function for the general population is best fit by a model with a clustering
length $r_0$=3.95$^{+0.48}_{-0.54}$ h$^{-1}$Mpc and slope
$\gamma$=1.8$^{+0.02}_{-0.06}$ at $z$~2.5, $r_0$=4.35$\pm$0.60 h$^{-1}$Mpc and
$\gamma$=1.6$^{+0.12}_{-0.13}$ at $z$~3.5. We use these clustering parameters
to derive the large-scale linear galaxy bias $b_L^{PL}$, between galaxies and
dark matter. We find $b_L^{PL}$ = 2.68$\pm$0.22 at redshift $z$~3 (assuming
$\sigma_8$ = 0.8), significantly higher than found at intermediate and low
redshifts. We fit an HOD model to the data and we obtain that the average halo
mass at redshift $z$~3 is $M_h$=10$^{11.75\pm0.23}$ h$^{-1}$M$_{\odot}$. From
this fit we confirm that the large-scale linear galaxy bias is relatively high
at $b_L^{HOD}$ = 2.82$\pm$0.27. Comparing these measurements with similar
measurements at lower redshifts we infer that the star-forming population of
galaxies at $z$~3 should evolve into the massive and bright ($M_r$<-21.5)
galaxy population which typically occupy haloes of mass $\langle M_h\rangle$ =
10$^{13.9}$ h$^{-1}$ $M_{\odot}$ at redshift $z$=0.
