The LCIR Survey, using the Cambridge IR Survey Instrument (CIRSI), reaches H ~ 20-21 over ~1 deg^2. We present results for 744 arcmin^2 in which public UBVRI data exist. We compare optical-IR colours with predictions of a semi-analytic hierarchical model (SAM) and find reasonable agreement. We also determine photometric redshifts, finding a median z of z_m ~ 0.55. We compare N(z) of different spectral types with models, showing that the observations are inconsistent with simple PLE models while the SAM provides a reasonable fit to the total N(z) but underestimates the number of z ~ 1 red spectral types. We also present N(z) for samples of red objects (EROs). We find that EROs with R - H > 4 and H < 20.5 have z_m ~ 1; redder EROs have higher z_m. For 19 < H < 20, EROs with R - H > 4 comprise ~18% of the observed galaxy population while in the SAM they contribute only ~4%. We also determine the angular correlation function w(theta) for magnitude, colour, spectral type and photo-z selected samples and use the estimated N(z) to derive the spatial clustering xi(r). Parametrizing xi(r) by xi(r_c,z)=(r_c/r_*(z))^(-1.8) (r_c comoving), we find that r_*(z) increases by ~1.5-2 times from z = 0 to z ~ 1.2. We interpret this as a selection effect - the galaxies selected at z ~ 1.2 are intrinsically very luminous. When galaxies are selected by absolute magnitude we find no evidence for evolution in r_* over this z range. Extrapolated to z = 0, we find r_*(0) ~ 6.5 h^-1Mpc for red galaxies and r_*(0) ~ 2-4 h^-1Mpc for blue galaxies. We also find that while the angular clustering amplitude of EROs with R - H > 4 or I - H > 3 is up to four times that of the whole galaxy population, the spatial clustering length r_*(z=1) is ~7.5-10.5 h^-1Mpc which is only a factor of ~1.7 times r_* for non-EROs lying in a similar z and luminosity range.
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