  We present new results on the young star population of the Lynds~1188
molecular cloud, associated with the Cepheus Bubble, a giant interstellar shell
around the association Cep~OB\,2. In order to reveal the star-forming scenario
of the molecular cloud located on the supershell, and understand the history of
star formation in the region, we identified and characterized young star
candidates based on an H$\alpha$ emission survey and various published
photometric datasets. Using Gaia DR2 astrometry we studied the spatial
distribution of the young star candidates and isolated three groups based on
their distances. We constructed spectral energy distributions of our target
stars, based on Pan-STARRS, 2MASS, {\it Spitzer} and {\it WISE} photometric
data, estimating their spectral types, extinctions, and luminosities. We
estimated masses by means of pre-main-sequence evolutionary models, and derived
accretion rates from the equivalent width of the H$\alpha$ line. We studied the
structure of the cloud by constructing a new extinction map, based on
Pan-STARRS data. Our results show that the distribution of low-mass young stars
in L1188 is well correlated with that of the dust and mole\-cular gas. We
identified two small, compact clusters and a loose aggregate of young stars. We
found that star formation in L1188 started about 5 million years ago. The
apparent age gradient of young stars across the cloud and the ammonia cores
located to the east of the optically visible young stellar groups support the
scenario of star formation propagating away from the centre of the Cepheus
Bubble.
