  We present the results of 20 ksec Chandra observations for each of 5 radio
galaxies in the redshift range 2.0 < z < 2.6. For 4 of the 5 targets we detect
unresolved X-ray components coincident with the radio nuclei. From spectral
analysis of one of the cores and comparison to the empirical radio to X-ray
luminosity ratio correlation, we find that obscuring material (n(HI)~10^22
cm^-2) may be surrounding the nuclei.
  We detect X-ray emission coincident with the radio hotspots or lobes in 4 of
the 5 targets, which can be explained by Inverse-Compton (IC) scattering of CMB
photons. The magnetic field strengths of ~100-200 muG that we derive agree with
the equipartition magnetic field strengths. The relative ease with which the
lobe X-ray emission is detected is a consequence of the (1+z)^4 increase in the
energy density of the CMB. An HST image of one of the sources shows that the
X-ray emission could also be produced by a reservoir of hot, shocked gas, as
evidenced by a bright, optical bow-shock.
  By stacking our data we created a deep, 100 ksec exposure to search for
diffuse X-ray emission from intra-cluster gas. We detect no diffuse emission
and derive upper limits of ~1e+44 erg/s, thereby ruling out a virialized
structure of cluster-size scale at z~2.
  The average number of soft X-ray sources in our fields is consistent with the
number density of AGN in the Chandra Deep Fields. Their angular distribution
shows no evidence for large-scale structure associated with the radio galaxies.
