  Galaxy models predict a tight relation between the clustering of galaxies and
dark matter on cosmological scales, but predictions differ notably in the
details. We used this opportunity and tested two semi-analytic models by the
Munich and Durham groups with data from the Canada-France-Hawaii Telescope
Lensing Survey (CFHTLenS). For the test we measured the scale-dependent galaxy
bias factor $b(k)$ and correlation factor $r(k)$ from linear to non-linear
scales of $k\approx10\,h\,\rm Mpc^{-1}$ at two redshifts $\bar{z}=0.35,0.51$
for galaxies with stellar mass between $5\times10^9$ and
$3\times10^{11}\,h_{\rm 70}^{-2}\,{\rm M}_\odot$. Our improved gravitational
lensing technique accounts for the intrinsic alignment of sources and the
magnification of lens galaxies for better constraints for the galaxy-matter
correlation $r(k)$. Galaxy bias in CFHTLenS increases with $k$ and stellar
mass, it is colour-dependent, revealing the individual footprints of galaxy
types. Despite a reasonable model agreement for the relative change with both
scale and galaxy properties, there is a clear conflict for $b(k)$ with no model
preference: the model galaxies are too weakly clustered. This may flag a model
problem at $z\gtrsim0.3$ for all stellar masses. As in the models, however,
there is a high correlation $r(k)$ between matter and galaxy density on all
scales, and galaxy bias is typically consistent with a deterministic bias on
linear scales. Only our blue and low-mass galaxies of about
$7\times10^9\,h_{\rm 70}^{-2}\,{\rm M}_\odot$ at $\bar{z}=0.51$ show, contrary
to the models, a weak tendency towards a stochastic bias on linear scales where
$r_{\rm ls}=0.75\pm0.14\,{\rm(stat.)}\pm0.06\,{\rm(sys.)}$. This result is of
interest for cosmological probes, such as $E_{\rm G}$, that rely on a
deterministic galaxy bias.
