  The brown dwarf population in the canonical star forming region NGC2264 is so
far poorly explored. We present a deep, multi-wavelength, multi-epoch survey of
the star forming cluster NGC2264, aimed to identify young brown dwarf
candidates in this region. Using criteria including optical/near-infrared
colours, variability, Spitzer mid-infrared colour excess, extinction, and Gaia
parallax and proper motion (in order of relevance), we select 902 faint red
sources with indicators of youth. Within this sample we identify 429 brown
dwarf candidates based on their infrared colours. The brown dwarf candidates
are estimated to span a mass range from 0.01 to 0.08$M_{\odot}$. We find
rotation periods for 44 sources, 15 of which are brown dwarf candidates,
ranging from 3.6 hours to 6.5 days. A subset of 38 brown dwarf candidates show
high level irregular variability indicative of ongoing disc accretion, similar
to the behaviour of young stars.
