  The amplitude of the angular two-point galaxy correlation function w(\theta)
for galaxies at z~2 is estimated for galaxies in the Hubble Deep Field by using
a U < 27 complete sub-sample.
  (i) It is confirmed that the amplitude of the correlation can be corrected
for the integral constraint without having to make assumptions about the shape
of the correlation function and by avoiding the introduction of linear error
terms. The estimate using this technique is w(5'') = 0.10 \pm 0.09.
  (ii) If the biases introduced in faint galaxy selection due to obscuration by
large objects are not corrected for by masking areas around them, then the
estimate would be w(5'') =0.16\pm 0.07.
  (iii) The effective (3-D) galaxy pair separation at 5'' and this redshift
range is ~ 25-250 /h kpc, so the correction to the spatial correlation function
\xi(r) due to exclusion of overlapping galaxy dark matter haloes should be
considered. For clustering stable in proper units in an \Omega=1,\lambda=0
universe, our w(5\arcs) estimate (a) implies a present-day correlation length
of r_0 ~ 2.6^{+1.1}_{-1.7}/h Mpc if halo overlapping is ignored, but (b) for a
present-day correlation length of r_0=5.5/h Mpc implies that a typical halo
exclusion radius is r_halo=70^{+420}_{-30}/h kpc.
  (iv) The decreasing correlation period (DCP) of a high initial bias in the
spatial correlation function is not detected at this redshift. For an
\Omega=1,\lambda=0 universe and (proper) stable clustering, possible detections
of the DCP in other work would imply that \xi at redshifts greater than z_t =
1.7\pm0.9 would be [(1+z)/(1+z_t)]^{2.1\pm3.6} times higher than at z_t, which
is consistent with our lack of a detection at z ~ 2.
