  Using the Chandra X-ray Observatory we have discovered a diffuse,
center-filled region of hard X-ray emission within the young, oxygen-rich
supernova remnant (SNR) G292.0+1.8. Near the peak of this diffuse emission lies
a point-like source of X-ray emission that is well described by an absorbed
power-law spectrum with photon index $1.72\pm0.09$. This source appears to be
marginally extended; its extent of 1.3$^{\prime\prime}$ (FWHM) is greater than
that of a nearby serendipitous X-ray source with FWHM = $1.1^{\prime\prime}$.
This is strong evidence for the presence within SNR G292.0+1.8 of a young
rapidly-rotating pulsar and its associated pulsar wind nebula. From the
unabsorbed, 0.2-4 keV band X-ray luminosity of the pulsar wind nebula ($L_X\sim
4\times 10^{34} \rm ergs s^{-1}$), we infer a spin-down energy loss rate of
$\dot E \sim 7\times 10^{36} \rm ergs s^{-1}$ for the still undetected pulsar.
The pulsar candidate is $0.9^\prime$ from the geometric center of the SNR which
implies a transverse velocity of $\sim$$770 (D/4.8 {\rm kpc}) (t/1600 {\rm
yr})^{-1} \rm km s^{-1}$ assuming currently accepted values for the distance
and age of G292.0+1.8.
