  Star-forming galaxies are a highly biased tracer of the underlying dark
matter density field. Their clustering can be studied through the cosmic
infrared background anisotropies. These anisotropies have been measured from
100 \mum to 2 mm in the last few years. In this paper, we present a fully
parametric model allowing a joint analysis of these recent observations. In
order to develop a coherent model at various wavelengths, we rely on two
building blocks. The first one is a parametric model that describes the
redshift evolution of the luminosity function of star-forming galaxies. It
compares favorably to measured differential number counts and luminosity
functions. The second one is a halo model based description of the clustering
of galaxies. Starting from a fiducial model, we investigate parameter
degeneracies using a Fisher analysis. We then discuss how halo of different
mass and redshift, how LIRGs and ULIRGs, contribute to the CIB angular power
spectra.
  From the Fisher analysis, we conclude that we cannot constrain the parameters
of the model of evolution of galaxies using clustering data only. The use of
combined data of C\ell, counts and luminosity functions improves slightly the
constraints but does not remove any degeneracies. On the contrary, the
measurement of the anisotropies allows us to set interesting constraints on the
halo model parameters, even if some strong degeneracies remain. Using our
fiducial model, we establish that the 1-halo and 2-halo terms are not sensitive
to the same mass regime. We also illustrate how the 1-halo term can be
misinterpreted with the Poisson noise term. Conclusions. We present a new model
of the clustering of infrared galaxies. However such a model has a few
limitations, as the parameters of the halo occupation suffer from strong
degeneracies.
