Abstract We have analyzed the data from a large-scale CO survey toward the northern region of the Small Magellanic Cloud (SMC) obtained with the Atacama Compact Array (ACA) stand-alone mode of ALMA. The primary aim of this study is to comprehensively understand the behavior of CO as an H₂ tracer in a low-metallicity environment (Z ∼ 0.2 Z _⊙). The total number of mosaic fields is ∼8000, which results in a field coverage of 0.26 deg² (∼2.9 ×10⁵ pc²), corresponding to ∼10% of the area of the galaxy. The sensitive ∼2 pc resolution observations reveal the detailed structure of the molecular clouds previously detected in the single-dish NANTEN survey. We have detected a number of compact CO clouds within lower H₂ column density (∼10²⁰ cm⁻²) regions whose angular scale is similar to the ACA beam size. Most of the clouds in this survey also show peak brightness temperature as low as <1 K, which for optically thick CO emission implies an emission size much smaller than the beam size, leading to beam dilution. The comparison between an available estimation of the total molecular material traced by thermal dust emission and the present CO survey demonstrates that more than ∼90% of H₂ gas cannot be traced by the low-J CO emission. Our processed data cubes and 2D images are publicly available.