  We measured stacked weak lensing cluster masses for a sample of 1325 galaxy
clusters detected by the RedGOLD algorithm in the Canada-France-Hawaii
Telescope Legacy Survey W1 and the Next Generation Virgo Cluster Survey at
$0.2<z<0.5$, in the optical richness range $10<\lambda<70$. After a selection
of our best richness subsample ($20<\lambda<50$), this is the most
comprehensive lensing study of a $\sim 100\%$ complete and $\sim 90\%$ pure
optical cluster catalogue in this redshift range, with a total of 346 clusters
in $\sim164~deg^2$. We test three different mass models, and our best model
includes a basic halo model, with a Navarro Frenk and White profile, and
correction terms that take into account cluster miscentering, non-weak shear,
the two-halo term, the contribution of the Brightest Cluster Galaxy, and an a
posteriori correction for the intrinsic scatter in the mass-richness relation.
With this model, we obtain a mass-richness relation of $\log{M_{\rm
200}/M_{\odot}}=(14.48\pm0.04)+(1.14\pm0.23)\log{(\lambda/40)}$ (statistical
uncertainties). This result is consistent with other published lensing
mass-richness relations. When compared to X-ray masses and mass proxies, we
find that on average weak lensing masses are $\sim 10\%$ higher than those
derived in the X-ray in the range $2\times10^{13}M_{\rm \odot}<E(z) M^{X}_{\rm
200}<2\times10^{14}M_{\rm \odot}$, in agreement with most previous results and
simulations. We also give the coefficients of the scaling relations between the
lensing mass and X-ray mass proxies, $L_X$ and $T_X$, and compare them with
previous results.
