Eclipsing binaries ( EBs ) provide critical laboratories for empirically testing predictions of theoretical models of stellar structure and evolution . Pre-main sequence ( PMS ) EBs are particularly valuable , both due to their rarity and the highly dynamic nature of PMS evolution , such that a dense grid of PMS EBs is required to properly calibrate theoretical PMS models . Analyzing multi-epoch , multi-color light curves for \sim 2400 candidate Orion Nebula Cluster ( ONC ) members from our Warm Spitzer Exploration Science Program YSOVAR , we have identified twelve stars whose light curves show eclipse features . Four of these 12 EBs are previously known . Supplementing our light curves with follow-up optical and near-infrared spectroscopy , we establish two of the candidates as likely field EBs lying behind the ONC . We confirm the remaining six candidate systems , however , as newly identified ONC PMS EBs . These systems increase the number of known PMS EBs by over 50 % , and include the highest mass ( \theta ^ { 1 } Ori E , for which we provide a complete set of well determined parameters including component masses of 2.807 and 2.797 M _ { \odot } ) and longest period ( ISOY J053505.71-052354.1 , P \sim 20 days ) PMS EBs currently known . In two cases ( \theta ^ { 1 } Ori E and ISOY J053526.88-044730.7 ) , enough photometric and spectroscopic data exists to attempt an orbit solution and derive the system parameters . For the remaining systems , we combine our data with literature information to provide a preliminary characterization sufficient to guide follow-up investigations of these rare , benchmark systems .