  The young radio pulsar J1124-5916 is associated with a Cas A like supernova
remnant G292.0+1.8. It powers a compact torus-like pulsar wind nebula with a
jet first detected in X-rays and then identified in the optical and
mid-infrared. We carried out deep near-infrared observations of the pulsar
field to identify the pulsar and its nebula in this range. The direct imaging
mode of the NACO adaptive optics instrument at the ESO VLT in the H and Ks
bands was used. In both bands we detected a faint, H=21.30(10) and
Ks=20.45(10), extended elliptical object, whose center position is consistent
with the X-ray position of the pulsar. The morphology of the object and the
orientation of its major axis are in a good agreement with those observed for
the pulsar torus-like nebula in the mid-infrared, optical, and X-rays. This
suggests that it is the near-infrared counterpart of the nebula. The measured
fluxes compiled with the data in other ranges show a complicated unabsorbed
power law spectrum of the torus-like nebula with several steep breaks between
the near-infrared and mid-infrared, the optical and X-rays, and possibly in the
mid-infrared. This implies a multiple relativistic particle population
responsible for the synchrotron emission of the nebula in different spectral
ranges. We have not resolved the pulsar counterpart from its nebula and place
only upper limits on its brightness, H >= 23.9$ and Ks >= 22.7. Based on that,
its contribution to the total near-infrared flux of the pulsar+nebula system is
<= 10%, which is comparable with the expected contribution in the optical.
