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We have monitored nearly a square degree in IC 1396A/Tr 37 over 21 epochsextending over 2014 - 2016 for sources variable in the JHK bands. In our data,65 +\- 8 % of previously identified cluster members show variations, comparedwith < 0.3% of field stars. We identify 119 members of Tr 37 on the basis ofvariability, forming an unbiased sample down to the brown dwarf regime. TheK-band luminosity function in Tr 37 is similar to that of IC 348 but shifted tosomewhat brighter values, implying that the K- and M-type members of Tr 37 areyounger than those in IC 348. We introduce methods to classify the causes ofvariability, based on behavior in the color-color and color-magnitude diagrams.Accretion hot spots cause larger variations at J than at K with substantialscatter in the diagrams; there are at least a dozen, with the most activeresembling EXors. Eleven sources are probably dominated by intervention of dustclumps in their circumstellar disks with color behavior indicating the presenceof grains larger than for interstellar dust, presumably due to grain growth intheir disks. Thirteen sources have larger variations at K than at J or H. For11 of them, the temperature fitted to the variable component is very close to2000K, suggesting that the changes in output are caused by turbulence at theinner rim of the circumstellar disk exposing previously protected populationsof grains.

Near-Infrared Variability of Low Mass Stars in IC 1396A and TR 37