  The initial conditions for the density perturbations in the early Universe,
which dictate the large scale structure and distribution of galaxies we see
today, are set during inflation. Measurements of primordial non-Gaussianity are
crucial for distinguishing between different inflationary models. Current
measurements of the matter power spectrum from the CMB only constrain this on
scales up to $k\sim 0.1$ Mpc$^{-1}$. Reaching smaller angular scales (higher
values of $k$) can provide new constraints on non-Gaussianity. A powerful way
to do this is by measuring the $\textrm{H}\textrm{I}$ matter power spectrum at
$z\gtrsim30$. In this paper, we investigate what values of $k$ can be reached
for the LOw Frequency ARray (LOFAR), which can achieve $\lesssim$1$''$
$\,$resolution at $\sim$50 MHz. Combining this with a technique to isolate the
spectrally smooth foregrounds to a wedge in $k_{\parallel}$ - $k_{\perp}$
space, we demonstrate what values of $k$ we can feasibly reach within
observational constraints. We find that LOFAR is $\sim$5 orders of magnitude
away from the desired sensitivity, for 10 years of integration time.
