  The intrinsic alignment (IA) of galaxies is potentially a major limitation in
deriving cosmological constraints from weak lensing surveys. In order to
investigate this effect we assign intrinsic shapes and orientations to galaxies
in the light-cone output of the MICE simulation, spanning $\sim5000\,{\rm
deg}^2$ and reaching redshift $z=1.4$. This assignment is based on a
'semi-analytic' IA model that uses photometric properties of galaxies as well
as the spin and shape of their host halos. Advancing on previous work, we
include more realistic distributions of galaxy shapes and a luminosity
dependent galaxy-halo alignment. The IA model parameters are calibrated against
COSMOS and BOSS LOWZ observations. The null detection of IA in observations of
blue galaxies is accounted for by setting random orientations for these
objects. We compare the two-point alignment statistics measured in the
simulation against predictions from the analytical IA models NLA and TATT over
a wide range of scales, redshifts and luminosities for red and blue galaxies
separately. We find that both models fit the measurements well at scales above
$8\,h^{-1}{\rm Mpc}$, while TATT outperforms NLA at smaller scales. The IA
parameters derived from our fits are in broad agreement with various
observational constraints from red galaxies. Lastly, we build a realistic
source sample, mimicking DES Year 3 observations and use it to predict the IA
contamination to the observed shear statistics. We find this prediction to be
within the measurement uncertainty, which might be a consequence of the random
alignment of blue galaxies in the simulation.
