  We present a novel simulation-based cosmological analysis of galaxy-galaxy
lensing and galaxy redshift-space clustering. Compared to analysis methods
based on perturbation theory, our simulation-based approach allows us to probe
a much wider range of scales, $0.4 \, h^{-1} \, \mathrm{Mpc}$ to $63 \, h^{-1}
\, \mathrm{Mpc}$, including highly non-linear scales, and marginalises over
astrophysical effects such as assembly bias. We apply this framework to data
from the Baryon Oscillation Spectroscopic Survey LOWZ sample cross-correlated
with state-of-the-art gravitational lensing catalogues from the Kilo Degree
Survey and the Dark Energy Survey. We show that gravitational lensing and
redshift-space clustering when analysed over a large range of scales place
tight constraints on the growth-of-structure parameter $S_8 = \sigma_8
\sqrt{\Omega_{\rm m} / 0.3}$. Overall, we infer $S_8 = 0.792 \pm 0.022$ when
analysing the combination of galaxy-galaxy lensing and projected galaxy
clustering and $S_8 = 0.771 \pm 0.027$ for galaxy redshift-space clustering.
These findings highlight the potential constraining power of full-scale studies
over studies analysing only large scales, and also showcase the benefits of
analysing multiple large-scale structure surveys jointly. Our inferred values
for $S_8$ fall below the value inferred from the CMB, $S_8 = 0.834 \pm 0.016$.
While this difference is not statistically significant by itself, our results
mirror other findings in the literature whereby low-redshift large scale
structure probes infer lower values for $S_8$ than the CMB, the so-called
$S_8$-tension.
