  The impact of biasing schemes on the clustering of tracers of the large-scale
structure is analytically studied in the weakly nonlinear regime. For this
purpose, we use the one-loop approximation of the integrated perturbation
theory together with the renormalized bias functions of various, physically
motivated Lagrangian bias schemes. These include the halo, peaks and excursion
set peaks model, for which we derive useful formulae for the evaluation of
their renormalized bias functions. The shapes of the power spectra and
correlation functions are affected by the different bias models at the level of
a few percent on weakly nonlinear scales. These effects are studied
quantitatively both in real and redshift space. The amplitude of the
scale-dependent bias in the presence of primordial non-Gaussianity also depends
on the details of the bias models. If left unaccounted for, these theoretical
uncertainties could affect the robustness of the cosmological constraints
extracted from galaxy clustering data.
