We present a preliminary analysis focusing on the hard tail observed in the X-ray spectroscopy of N132D, a young shell-like supernova remnant (SNR) in the Large Magellanic Cloud. The data we used are two Chandra HETG zeroth-order data obtained in 2000, with exposure time of 22 and 74 ks respectively. Though two distinctive models(an additive non-thermal or thermal component) can both explain the hard tail well, and are both statistically adequate, we find that the existence of the hard tail is highly consistent with the density of ISM. That is to say, this hard tail is more likely to show up when the surrounding ISM is denser. Based on this view, a non-thermal component may be the major source of the hard tail.