  Observations of low-mass stars have frequently shown a disagreement between
observed stellar radii and radii predicted by theoretical stellar structure
models. This ``radius inflation'' problem could have an impact on both stellar
and exoplanetary science. We present the final results of our observation
programme with the CHEOPS satellite to obtain high-precision light curves of
eclipsing binaries with low mass stellar companions (EBLMs). Combined with the
spectroscopic orbits of the solar-type companion, we can derive the masses,
radii and effective temperatures of 23 M-dwarf stars. We use the PYCHEOPS data
analysis software to analyse their primary and secondary occultations. For all
but one target, we also perform analyses with TESS light curves for comparison.
We have assessed the impact of starspot-induced variation on our derived
parameters and account for this in our radius and effective temperature
uncertainties using simulated light curves. We observe trends for inflation
with both metallicity and orbital separation. We also observe a strong trend in
the difference between theoretical and observational effective temperatures
with metallicity. There is no such trend with orbital separation. These results
are not consistent with the idea that observed inflation in stellar radius
combines with lower effective temperature to preserve the luminosity predicted
by low-mass stellar models. Our EBLM systems are high-quality and homogeneous
measurements that can be used in further studies into radius inflation.
