  The gravitational wave emission from the merging binary neutron star system
GW170817 arrived full of tidal information which can be used to probe the
fundamental ultra-dense nuclear physics residing in these stars. In previous
work, we used two-dimensional correlations between nuclear matter parameters
and tidal deformabilities of neutron stars applying specifically to GW170817 to
derive constraints on the former. Here, we extend this analysis by finding
similar correlations for varying chirp masses, the dominant determining factor
in the frequency evolution of the inspiral, such that one can apply the same
method to future detections. We estimate how accurately one can measure nuclear
parameters with future gravitational wave interferometers and show how such
measurements can be improved by combining multiple events. We find that bounds
on the nuclear parameters with future observations can improve from the current
one with GW170817 only by $\sim 30\%$ due to the existence of systematic errors
caused mainly by the remaining uncertainty in the equation of state near and
just above the nuclear saturation density. We show that such systematic errors
can be reduced by considering multidimensional correlations among nuclear
parameters and tidal deformabilities with various neutron star masses.
