This paper presents a method to distinguish between bound and unbound open clusters (OCs) using their masses and Jacobi radii. The authors use Gaia DR3 data to create a cleaned star cluster catalogue, which includes 3530 open clusters in a high-quality sample. They find that only 79% of the clusters in their previous catalogue are compatible with being bound OCs, with 11% within 250 pc. The authors also show that the mass-dependent completeness of the open cluster census is only reliable for objects heavier than 230 M☉, and that the Milky Way contains approximately 1.3 × 10⁵ open clusters, of which only 4% are currently known. The authors demonstrate that most open clusters have mass functions compatible with the Kroupa initial mass function. They also show that the Jacobi radius is a useful tool for distinguishing between bound and unbound clusters, and that their updated catalogue includes masses and improved classifications. The authors also correct for selection effects and unresolved binary stars in their mass calculations, and show that their method is computationally feasible for future cluster blind searches. The results show that the majority of clusters in the solar neighbourhood are classified as moving groups (MGs), with only a small fraction being true OCs. The authors also highlight the importance of using a minimum Jacobi mass of 40 M☉ when distinguishing between OCs and MGs. The final catalogue includes 5647 clusters with P(r_J) > 0.5, a minimum mass of 40 M☉, and at least ten observed stars within r_J. The authors also provide updated classifications and names for several clusters, including those classified as globular clusters (GCs). The results show that the majority of clusters in the solar neighbourhood are classified as MGs, with only a small fraction being true OCs. The authors also highlight the importance of using a minimum Jacobi mass of 40 M☉ when distinguishing between OCs and MGs. The final catalogue includes 5647 clusters with P(r_J) > 0.5, a minimum mass of 40 M☉, and at least ten observed stars within r_J.This paper presents a method to distinguish between bound and unbound open clusters (OCs) using their masses and Jacobi radii. The authors use Gaia DR3 data to create a cleaned star cluster catalogue, which includes 3530 open clusters in a high-quality sample. They find that only 79% of the clusters in their previous catalogue are compatible with being bound OCs, with 11% within 250 pc. The authors also show that the mass-dependent completeness of the open cluster census is only reliable for objects heavier than 230 M☉, and that the Milky Way contains approximately 1.3 × 10⁵ open clusters, of which only 4% are currently known. The authors demonstrate that most open clusters have mass functions compatible with the Kroupa initial mass function. They also show that the Jacobi radius is a useful tool for distinguishing between bound and unbound clusters, and that their updated catalogue includes masses and improved classifications. The authors also correct for selection effects and unresolved binary stars in their mass calculations, and show that their method is computationally feasible for future cluster blind searches. The results show that the majority of clusters in the solar neighbourhood are classified as moving groups (MGs), with only a small fraction being true OCs. The authors also highlight the importance of using a minimum Jacobi mass of 40 M☉ when distinguishing between OCs and MGs. The final catalogue includes 5647 clusters with P(r_J) > 0.5, a minimum mass of 40 M☉, and at least ten observed stars within r_J. The authors also provide updated classifications and names for several clusters, including those classified as globular clusters (GCs). The results show that the majority of clusters in the solar neighbourhood are classified as MGs, with only a small fraction being true OCs. The authors also highlight the importance of using a minimum Jacobi mass of 40 M☉ when distinguishing between OCs and MGs. The final catalogue includes 5647 clusters with P(r_J) > 0.5, a minimum mass of 40 M☉, and at least ten observed stars within r_J.