  We test the regime of validity of one-loop galaxy bias for a wide variety of
biased tracers. Our most stringent test asks the bias model to simultaneously
match the galaxy-galaxy and galaxy-mass spectrum, using the measured nonlinear
matter spectrum from the simulations to test one-loop effects from the bias
expansion alone. In addition, we investigate the relevance of short-range
nonlocality and halo exclusion through higher-derivative and scale-dependent
noise terms, as well as the impact of using co-evolution relations to reduce
the number of free fitting parameters. From comparing validity and merit of
these assumptions we find that a four-parameter model (linear, quadratic, cubic
nonlocal bias, and constant shot noise) with fixed quadratic tidal bias
provides a robust modeling choice for the auto power spectrum of the less
massive halos in our set of samples and their galaxy populations (up to
$k_{\mathrm{max}} = 0.35\,h/\mathrm{Mpc}$ for a sample volume of
$6\,(\mathrm{Gpc}/h)^3$). For the more biased tracers it is most beneficial to
include scale-dependent noise. This is also the preferred option when
considering combinations of the auto and cross power spectrum, which might be
relevant in joint studies of galaxy clustering and weak lensing. We also test
the use of perturbation theory to account for matter loops through gRPT, EFT
and the hybrid approach RESPRESSO. While all these have similar performance, we
find the latter to be the best in terms of validity and recovered mean
posterior values, in accordance with it being based partially on simulations.
