  We study the evolution of galaxy clustering in various cosmological models
with quintessence. We investigate how the analytical predictions vary with
change of dark energy equation of state $w_X$. Comparing these predictions
against available data we discuss to what extent the problems of galaxy biasing
can be modelled. This will be key in constraining the dark energy equation of
state with future galaxy surveys. We use a compilation of various surveys to
study the number density and amplitude of galaxy clustering from observations
of the local universe at $z \sim 0$ to that of the Lyman break galaxies and
Ly-$\alpha$ emitters at $z \sim 4.9$. We find that there is a degeneracy
between the dark energy equation of state and the way galaxies populate dark
matter haloes; objects are more biased in models with more negative values of
dark energy equation of state $w_X$.
  We conclude that, while future all sky CMB observations will determine
cosmological parameters with unprecedented precision, and cross correlation of
weak lensing experiments and galaxy surveys will provide a cleaner and accurate
picture of bias associated with collapsed objects, the rate of growth of large
scale structure in such surveys can potentially constrain the equation of state
of dark energy and the potential of the scalar field associated with
quintessence. In particular, we show that the abundance and spatial
distribution of galaxy clusters at intermediate redshifts strongly depend on
the dark energy equation of state. When accurate measurement of galaxy
clustering at high-redshit becomes possible, it will provide constraints on
dark energy that are independent and complementary to type Ia supernova
studies.
