HI emission and absorption line studies with the ATCA reveal a surprisingly high fraction of cool HI gas in the LMC. No CO has been detected in most of these regions, which show unusually low temperatures down to 4 K. Therefore, we are faced with a numerous population of dense and cold clouds, which consist primarily of atomic neutral hydrogen. These clumps may be a key to understand the high star formation activity in the LMC. The cooling mechanism of these clouds, some of which are located in warm surroundings, is, however, still an open question. The resolution and sensitivity of the ISO telescope offers a unique opportunity to study the heating/cooling balance of these clouds in the LMC. Therefore, we propose to observe the dominant cooling lines [CII], [OI], and [NII] to achieve this scientific goal as a further step towards the understanding of star formation in the LMC.