  We study a sample of ~10^4 galaxy clusters in the redshift range 0.2<z<0.8
with masses M_200 > 5x10^13 h_70^-1 M_sun, discovered in the second
Red-sequence Cluster Survey (RCS2). The depth and excellent image quality of
the RCS2 enable us to detect the cluster-mass cross-correlation up to z~0.7. To
obtain cluster masses, concentrations and halo biases, we fit a cluster halo
model simultaneously to the lensing signal and to the projected density profile
of red-sequence cluster members, as the latter provides tight constraints on
the cluster miscentring distribution. We parametrise the mass-richness relation
as M_200 = A x (N_200/20)^alpha, and find A = (15.0 +- 0.8) x 10^13 h_70^-1
M_sun and alpha = 0.73 +- 0.07 at low redshift (0.2<z<0.35). At intermediate
redshift (0.35<z<0.55), we find a higher normalisation, which points at a
fractional increase of the richness towards lower redshift caused by the
build-up of the red-sequence. The miscentring distribution is well constrained.
Only ~30% of our BCGs coincide with the peak of the dark matter distribution.
The distribution of the remaining BCGs are modelled with a 2D-Gaussian, whose
width increases from 0.2 to 0.4 h_70^-1 Mpc towards higher masses; the ratio of
width and r_200 is constant with mass and has an average value of 0.44 +- 0.01.
The mass-concentration and mass-bias relation agree fairly well with literature
results at low redshift, but have a higher normalisation at higher redshifts,
which may be due to selection and projection effects. The concentration of the
satellite distribution decreases with mass and is correlated with the
concentration of the halo.
