  Surveys of cosmological large-scale structure (LSS) are sensitive to the
presence of local primordial non-Gaussianity (PNG), and may be used to
constrain models of inflation. Local PNG, characterized by fNL, the amplitude
of the quadratic correction to the potential of a Gaussian random field, is
traditionally measured from LSS two-point and three-point clustering via the
power spectrum and bi-spectrum. We propose a framework to measure fNL using the
configuration space two-point correlation function (2pcf) monopole and
three-point correlation function (3pcf) monopole of survey tracers. Our model
estimates the effect of the scale-dependent bias induced by the presence of PNG
on the 2pcf and 3pcf from the clustering of simulated dark matter halos. We
describe how this effect may be scaled to an arbitrary tracer of the
cosmological matter density. The 2pcf and 3pcf of this tracer are measured to
constrain the value of fNL. Using simulations of luminous red galaxies observed
by the Dark Energy Spectroscopic Instrument (DESI), we demonstrate the accuracy
and constraining power of our model, and forecast the ability to constrainfNL
to a precision of sigma(fNL) = 22 with one year of DESI survey data.
